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Solution of Vacuum Field Equation Based on Physics Metrics in Finsler Geometry and Kretschmann Scalar

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Solution of Vacuum Field Equation Based on Physics Metrics in Finsler Geometry and Kretschmann Scalar Archive of SID Int. J. Nonlinear Anal. Appl. 10 (2019) Special Issue (Nonlinear Analysis in Engineering and Sciences), 97-114 ISSN: 2008-6822 (electronic) https://dx.doi.org/10.22075/IJNAA.2019.4403 Solution of Vacuum Field Equation Based on Physics Metrics in Finsler Geometry and Kretschmann Scalar M. Farahmandy Motlagh∗, A. Behzadi Department of Mathematics, Faculty of Basic Sciences, University of Mazandaran, P. O. Box 47416-95447, Babolsar, Iran. Abstract The Lemaître-Tolman-Bondi (LTB) model represents an inhomogeneous spherically symmetric uni- verse filled with freely falling dust like matter without pressure. First, we have considered a Finslerian anstaz of (LTB) and have found a Finslerian exact solution of vacuum field equation. We have ob- tained the R(t; r) and S(t; r) with considering establish a new solution of Rµν = 0. Moreover, we attempt to use Finsler geometry as the geometry of spacetime which compute the Kretschmann scalar. An important problem in General Relativity is singularities. The curvature singularities is a point when the scalar curvature blows up diverges. Thus we have determined Ks singularity is at R = 0. Our result is the same as Reimannian geometry. We have completed with a brief example of how these solutions can be applied. Second, we have some notes about anstaz of the Schwarzschild and Friedmann- Robertson- Walker (F RW ) metrics. We have supposed condition d log(F ) = d log(F¯) and we have obtained F¯ is constant along its geodesic and geodesic of F . Moreover we have com- 2 puted Weyl and Douglas tensors for F and have concluded that Rijk = 0 and this conclude that 2 2 Wijk = 0, thus F is the Ads Schwarzschild Finsler metric and therefore F is conformally flat. We have provided a Finslerian extention of Friedmann- Lemaitre- Robertson- Walker metric based on solution of the geodesic equation. Since the vacuum field equation in Finsler spacetime is equivalent to the vanishing of the Ricci scalar, we have obtained the energy- momentum tensor is zero. Keywords: Einstein’s equations, Lemaître–Tolman–Bondi; Kretschmann scalar, Finsler Geometry, Friedmann-Robertson-Walker, Schwarzschild. 1. Introduction Cosmic structures today have entered the non-linear structure. They can not on all scales be described by a linear perturbation theory on top of the Friedmann-Lemaitre-Robertson-Walker (FLRW) metric ∗Corresponding author Email address: [email protected], [email protected] (M. Farahmandy Motlagh∗, A. Behzadi) Received: July 2019 Revised: October 2019 www.SID.ir 98Archive of SID M. Farahmandy Motlagh, A. Behzadi [1]. Lemaitre-Tolman-Bondi (LTB) solutions are used frequently to describe the collapse or expansion of spherically symmetric inhomogeneous mass distributions in the Universe. The LTB solutions contain as special cases both the Schwazchild and dust FLRW solutions. The LTB metric is the simplest spherically symmetric solution of Einstein equations representing an inhomogeneous dust distribution. It may be written in synchronous coordinates as [2]: 0 2 R F 2 = −ytyt + ( )yryr + R2(r; t)(yθyθ + sinθy'y'); 1 + E The Kretschmann scalar gives the amount of curvature of spacetime, as a function of position near (and within) a black hole [3]. In many cases one of the most useful ways to check that is by checking for the finiteness of the Kretschmann scalar. The alternative way to describe the black holeswithin the cosmological surrounding is to use the Lemaitre-Tolman-Bondi (LTB) models for inhomogeneous matter distribution that was fundamentally explored in [4]. There are very few exact solutions of the Einstein equations, but perhaps the most well-known so- lution was first derived by Schwarzschild. Exact solutions of Einstein’s field equations have played important roles in the discussion of physical problems. Obvious examples are the Schwarzschild and Kerr solutions for studying black holes and the Friedman solutions for cosmology [5]. Gravitational field equations describing the geometry of space-time play a fundamental role inmod- ern theoretical physics. There are many methods in mathematical physics for studying such systems of equations. For example, one can use methods of additional symmetries of the system of equations, the Hamiltonian formulation of the theory of dynamical systems, etc. Essentially, all physically interesting cases (F RW cosmology, black hole) belong to Stackel and homogeneous spaces [6] In contrast, the cosmic fluid in the F RW model is supposed to possess arbitrary high pressure apart from arbitrary high density. But there is no pressure gradient to support the fluid against its self- gravity [7]. The paper is organized as follows. We review some basic matterial of Finsler geometry and list of tools that is needed in context. In section III we establish a new solution of Rµν = 0 which appears curious and explains the source of curvature of the well-known Lemaître–Tolman–Bondi(LTB) solu- tion. Moreover, we have analytic solution to the geodesic equations. In the section V we compute Kretschmann scalar and show that the LTB singularity is at R = 0. In the section VI we obtain Kretschmann scalar for a one example. The section VII presents opinion of Li and Chang [8] to other words. We consider an ansatz of the Schwarzschild metric F 2 and we show results of vacuum solution. In the section VIII, we compute Weyl and Douglas tensors for F 2 and conclude that 2 Rijk = 0 and this conclude that Wijk = 0, thus F is the Ads Schwarzschild Finsler metric and therefore F 2 is conformally flat. Then we consider Douglas tensor if D = 0 we conclude that F 2 is the Schwarzschild metric. In the section IX, we consider F LRW metric that it has the Finslerian structure then if only we suppose that the radial motion of particles, and notice the velocity of a dr particle is small, therefore the energy-momentum tensor is zero. dt 2. Preliminaries We begin with a very brief discussion of Finsler geometry. A Finsler metric is a continuous function F : TM ! [0; 1] with the following properties. (1) Regularity: F is smooth on TM n 0 := f(x; y) 2 TMjy =6 0g. (2) Positive homogeneity: F (x; λy) = λF (x; y) for all λ > 0. www.SID.ir Solution of Vacuum Field Equation Based on Physics Metrics in Finsler ... 10Archive (2019) Special of SID Issue (Nonlinear Analysis in Engineering and Sciences), 97-114 99 @ @ 1 2 (3) Strong convexity: the fundamental tensor gij := @yi @yj ( 2 F ). is positive definite at all (x; y) 2 TM n 0 [9]. A positive, zero and negative F correspond to time-like, null and space-like curves, respectively. For a Finsler metric F = F (x; y) its geodesics are characterized by the system of differential equations d2xµ + 2Gµ = 0; (2.1) dτ 2 Where the local functions Gµ = Gµ(x; y) are called the spray coefficients and are given by 1 @2F 2 @F 2 Gµ = gµν( yλ − ); (2.2) 4 @xλ@yν @xν µν −1 Where y 2 TxM and (g ) := (gµν) . The Cartan tensor quantifies, the deviation of F from being Riemannian, and is defined as @ @ @ 1 A := ( F 2); (2.3) ijk @yi @yj @yk 4 Where the components Aijk are minus one-homogeneous symmetric (0; 3)-tensor field. In order to calculate the Kretschmamm scalar, we need first to calculate the Christoffel symbols by differentiating the metric of F . 1 δg δg δg Γµ = gµl( lσ + lν − σν ); (2.4) νσ 2 δxν δxσ δxl δ @ − @Gρ @ where δxµ = @xµ @yµ @yρ : In Finsler geometry once the Christoffel symbols are calculated then we calculate the Riemann curvature of Chern connection to be: δΓµ δΓµ Rµ = νλ − νσ + Γl Γµ − Γl Γµ ; (2.5) νσλ δxσ δxλ νλ lσ νλ lλ λ From the Riemann tensor R νρσ one can calculate the Riemann curvature tensor Rµνρσ as follows: λ Rµνρσ = gµλR νρσ; (2.6) The inverse of Rµνρσ can be compute by µνρσ µi νj ρk σl R = g g g g Rijkl; (2.7) The Kretschmann invariant is µνρσ Ks = R Rµνρσ (2.8) Because it is a sum of squares of tensor components, this is a quadratic invariant. For the use of a computer algebra system a more detailed writing is meaningful: µi νj ρk σl Ks = g g g g RijklRµνρσ; (2.9) The Ricci tensor Rµν, it is the Riemann curvature tensor with the first and third indices contracted, αβ β Rµν = g Rαµβν = Rµβν; Which is a symmetric tensor, Rµν = Rνµ; www.SID.ir 100Archive of SID M. Farahmandy Motlagh, A. Behzadi It is straightforward to show that, because of the symmetry relations, the alternative contraction leads to the same Ricci tensor αβ Rµν = −g Rµαβν; The Ricci scalar R, it is the Riemann curvature tensor contracted twice. αβ β R = g Rαβ = Rβ; By definition, the Ricci scalar is a positively homogeneous function of degree twoin y 2 TM. For a Finsler metric F , the S−curvature is given by following: µν S = g Ricµν; (2.10) and, as a consequence, the modified Einstein tensor in Finsler space time can be obtained as 1 G ≡ Ric − g S; (2.11) µν µν 2 µν µ The covariant derivative of Gν in Finsler spacetime is given as δ Gµ = Gµ + Γµ Gρ − Γρ Gµ; (2.12) νjk δxk ν kρ ν kν ρ µ 0j0 Γkρ is the Chern connection and to denote the covariant derivative. Here, we consider also the Rici scalar which is expressed entirely in terms of x and y derivatives of spray coefficients Gµ as follows: @Gµ @2Gµ @2Gµ @Gµ @Gλ RicF 2 = 2 − yλ + 2Gλ − ; (2.13) @xµ @xλ@yµ @yλ@yµ @yλ @yµ 3. Vacuum solution of Finsler metric by using Ansatz of the LTB The theory of relativity describes the relation between the curvature of spacetime to the energy of an object.
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